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Some supernova (SN) explosions show evidence for interaction withpre-existing non-spherically symmetric circumstellar medium (CSM) in theirlight curves, spectral line profiles, and polarization signatures. To betterunderstand the connection with binary stars and to aid in the interpretation ofobservations, we perform two-dimensional axisymmetric hydrodynamic simulationswhere an expanding spherical SN ejecta initialized with realistic density andvelocity profiles collide with various aspherical CSM distributions. Weconsider CSM in the form of a circumstellar disk, colliding wind shells inbinary stars with different orientations and distances from the SN progenitor,and bipolar lobes representing a scaled down version of the Homunculus nebulaof $\eta$~Car. We study how our simulations map onto observables, includingapproximate light curves, indicative spectral line profiles at late times, andestimates of polarization signature. We find that the SN--CSM collision layeris composed of normal and oblique shocks, reflected waves, and otherhydrodynamical phenomena that lead to acceleration and shear instabilities. Asa result, the total shock heating power fluctuates in time, although theemerging light curve might be smooth if the shock interaction region is deeplyembedded in the SN envelope. SNe with circumstellar disks or bipolar lobesexhibit late-time spectral line profiles symmetric with respect to the restvelocity and relatively high polarization. In contrast, SNe with colliding windshells naturally lead to line profiles with asymmetric and time-evolving blueand red wings and low polarization. Given the high frequency of binaries amongmassive stars, interaction of SN ejecta with a pre-existing colliding windshell must occur and the observed signatures could be used to characterize thebinary companion.

Supernova explosions interacting with aspherical circumstellar material: implications for light curves, spectral line profiles, and polarization